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The Physics of the Solar Corona and Transition Region - Oddbjorn Engvold

The Physics of the Solar Corona and Transition Region

By: Oddbjorn Engvold (Editor), John W. Harvey (Editor), C. J. Schrijver (Editor), Neal E. Hurlburt (Editor)


Published: June 2001
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The Sun's magnetic field is responsible for the spectacularly dynamic and intricate phenomenon that we call the corona. The past decade has seen an enormous increase in our understanding of this part of the solar outer atmosphere, both as a result of observations and because of rapid advances in numerical studies. The YOHKOH satellite has observed the Sun now for over six years, producing spectacular sequences of images that convey the complexity of the corona. The imaging and spectroscopic instruments on SOHO have added information on the cooler part of the corona. And since April of 1998 TRACE has given us very high resolution images of the 1-2 MK corona, at cadences that allow detailed observations of field oscillations, loop evolution, mass ejecta, etc. This volume contains papers contributed to a workshop (held in August 1999 in Monterey, California) that was dedicated to an exploration of the most recent results on the solar corona, as well as on the transition region and low solar wind. The diverse presentations at the meeting revolved around one key theme: the entire outer atmosphere of the Sun is intrinsically dynamic, evolving so rapidly that even the concept of a single local temperature for a single fluid often breaks down. Moreover, the corona is an intrinsically nonlinear and nonlocal medium. These aspects are discussed in these proceedings that include both papers that review recent developments (both based on observations and on theoretical/numerical modeling), and original research papers based on observations from many different observatories. The papers presented at the meeting add up to such a volume that they are distributed over two Topical Issues of Solar Physics (December 1999 and April 2000), which are reprinted in these bound volumes, of which this is the second.

Three-Dimensional Separator Reconnection - How Does It Occur?
The Structure of Force-Free Magnetic Fields
Models of Dynamic Coronal Loops
Cross-Sectional Properties of Coronal Loops
Width Variations along Coronal Loops Observed by TRACE
How Accurately Can We Determine the Coronal Heating Mechanism in the Large-Scale Solar Corona?
SERTS-97 Measurement of Relative Wavelength Shifts in Coronal Emission Lines across a Solar Active Region
Modeling Coronal Loop Abundances: Effects of Parameter Variations on Observables
Waves and Oscillations in the Corona
Can Gravitational Effects Damp AlfvFn Waves?
Observations of the 24 September 1997 Coronal Flare Waves
Structure of a Large Low-Latitude Coronal Hole
Electro-Mechanical Coupling between the Photosphere and Transition Region
The Magnetic Connectivity of Moss Regions
Magnetic Activity Associated with Radio Noise Storms
A Kinetic Model of Coronal Heating and Acceleration by Ion-Cyclotron Waves: Preliminary Results
SECIS: The Solar Eclipse Coronal Eclipse Imaging System
The SOHO-Stellar Connection
Table of Contents provided by Publisher. All Rights Reserved.

ISBN: 9780792370437
ISBN-10: 0792370430
Audience: Professional
Format: Hardcover
Language: English
Number Of Pages: 392
Published: June 2001
Country of Publication: NL
Dimensions (cm): 23.39 x 15.6  x 2.24
Weight (kg): 0.74